藉散斑遮罩技術重建雙星影像

Image Reconstruction of Selected Binaries by Speckle-Masking Method

鄭憲隆(Hsien-Lung Cheng)

指導教授 ： 傅學海

國立臺灣師範大學/理學院/地球科學系/碩士(2012年)

摘要

散斑干涉法是觀測雙星的一種普遍方法，臺師大於2006年開始推動雙星散斑干涉。觀測的雙星選自美國海軍天文台的華盛頓雙星星表，其中觀測目標之伴星星等小於6等，雙星亮度差異小於5等，雙星角距介於0.4到4角秒之間。
但是散斑干涉法在利用傅立葉轉換取得雙星位置時會產生鏡向影像，這對小角距雙星的方位角判別將會產生困擾，並且會失去雙星的亮度資訊。
因此，在此論文中引用了Weigelt在1977年提出的散斑遮罩影像重建法來還原雙星影像。研究結果顯示，此方法之效益相當好，可以有效還原雙星之亮度差異資訊，測量雙星之角距與方位角，以求得軌道參數、雙星質量等訊息。未來如果能夠加入不同波段濾鏡所得到之亮度差異，可以得到雙星的溫度資訊，進而討論雙星演化過程。

關鍵字：雙星、散斑、影像重建

關鍵字

雙星 ； 散斑 ； 影像重建

並列摘要

This speckle observation program began since 2006 in NTNU, and the binaries were selected from Washington Double Star (WDS) catalog, USNO, with their V magnitude of secondary brighter than 6, magnitude difference between primary and secondary smaller than 5, and their angular separations between 0.4″ and 4″.
By using the method of Fast Fourier Transform or autocorrelation to find the information of the relational position between th3 primary and the secondary, but, there are no the information of intensity and amplitude of stellar light.
In this work, the speckle-masking method, developed by Weigelt in 1977, is used to reconstruct the distribution of intensity of primary and secondary. .
From the reconstructed image with the method of speckle-masking, the magnitude difference of the binaries will be calculated. With the magnitude of binary (primary and secondary mixing in the seeing disk) taken from literature, the magnitude of the primary and the secondary will be calculated, respectively. And furthermore, if the magnitude difference in B and V band could be obtained, the temperature information could be used to discuss the binary systems evolution.

Keyword: Binary, Speckle, Image reconstruction

並列關鍵字

Binary ； Speckle ； Image reconstruction

參考文獻

Scardia, Marco, Argyle, Robert, Prieur, Jean-Louis, Pansecchi, Luigi, Basso, Stefano, Law, Nicholas, Mackay, Craig, 2007, IAUS, 240,558S.

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McAlister, Harold A.; Hartkopf, William I.; Hutter, Donald J.; Franz, Otto G., 1987AJ, 93, 688M

Bonneau, D., Foy, R., 1980, A&A, 86, no. 3, 295.

Hartkopf, W. I., McAlister, H. A., 1991, Astrophysics and Space Science, 177, no. 1-2, 161.